The assumption of circular orbits for candidate signals of the three planets can be justified by considering the tidal circularization timescales. According to [1]} we could assume negligible eccentricities for the signals at 0.85 and 3.69 days, having periods less than 6 days and hence accounted for by dissipation of tidal disturbances within their envelopes that are induced by their host stars. For the third signal at a period of 8.96 days, we calculated the circularization timescale as described in [1]}, and found a value of \(\sim \) 610 Gyr for an assumed planetary tidal quality factor \(Q_p^{\prime } = 10^6\) . We also relaxed the prior on eccentricity for the analysis in Section REF  to allow the data to find the feasible value. The obtained value for eccentricity falls around 0.057±0.062 (see Figure REF ), again supporting the assumption of circular orbits.
